AAS 201st Meeting, January, 2003
Session 79. Intergalactic Material: Its Structure and Composition
Poster, Wednesday, January 8, 2003, 9:20am-6:30pm, Exhibit Hall AB

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[79.11] Intergalactic Dust

A. Li (University of Arizona)

We study the composition and sizes of intergalactic dust based on the expulsion of interstellar dust from the galactic disk. Interstellar grains in the Galactic disk are modelled as a mixture of amorphous silicate dust and carbonaceous dust consisting of polycyclic aromatic hydrocarbon (PAH) molecules and larger graphitic grains (Li & Draine 2001) with size distributions like those of the Milky Way dust (Weingartner & Draine 2001). We model their dynamic evolution in terms of the collective effects caused by (1) radiative acceleration, (2) gravitational attraction, (3) gas drag, (4) thermal sputtering, and (5) Lorenz force from the galactic magnetic field (Ferrara et al. 1991). Radiation pressure from the stellar disk exerts an upward force on dust grains and may ultimately expel them out of the entire galaxy. Gravitational force from the stellar, dust and gas disk as well as the dark matter halo exerts a downward force. Thermal sputtering erodes all grains to some degree but more efficiently destroys small grains. This, together with the fact that (1) very small grains (with small radiation pressure efficiencies) are not well coupled to starlight; (2) for large grains the radiative force to the gravitational force is approximately inversely proportional to grain size, acts as a size ``filter'' for dust leaking into the intergalactic space. Since the radiation pressure efficiency and the grain destruction rate are sensitive to dust composition, the relative importance of carbon dust compared to silicate dust expelled into the intergalactic space differs from that in the galactic plane.

We derive the size distributions of both silicate and carbonaceous dust finally getting into the intergalactic space and obtain an intergalactic extinction curve. The predicted intergalactic infrared emission spectrum is calculated.\\

References: \\ Ferrara, A., Ferrini, F., Franco, J., & Barsella, B. 1991, ApJ, 381, 137\\ Li, A., & Draine, B.T. 2001, ApJ, 554, 778\\ Weingartner, J.C., & Draine, B.T. 2001, ApJ, 548, 296\\

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The author(s) of this abstract have provided an email address for comments about the abstract: agli@lpl.arizona.edu

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